2008
DOI: 10.1111/j.1365-2966.2008.13923.x
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Altitude-dependent polarization in radio pulsars

Abstract: Because of the corotation, the polarization angle (PA) curve of a pulsar lags the intensity profile by 4r/Rlc rad in pulse phase. I present a simple and short derivation of this delay-radius relation to show that it is not caused by the aberration (understood as the normal beaming effect) but purely by contribution of corotation to the electron acceleration in the observer's frame. Available altitude-dependent formulae for the PA curve are expressed through observables and emission altitude to make them immedi… Show more

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Cited by 52 publications
(73 citation statements)
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References 39 publications
(53 reference statements)
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“…We can think of two viable alternatives in this scenario: either (1) adapt or modify the BCW91 formulation for a variable emission altitude r (Dyks 2008) or (2) fit the BCW91 curve for regions of the PPA profile having a relatively constant value of r. We prefer the latter alternative to evade the modification of the theory behind the BCW91 model. Here we note that α and β are not invoked as fit parameters; instead we used their published values in Eq.…”
Section: Resultsmentioning
confidence: 99%
“…We can think of two viable alternatives in this scenario: either (1) adapt or modify the BCW91 formulation for a variable emission altitude r (Dyks 2008) or (2) fit the BCW91 curve for regions of the PPA profile having a relatively constant value of r. We prefer the latter alternative to evade the modification of the theory behind the BCW91 model. Here we note that α and β are not invoked as fit parameters; instead we used their published values in Eq.…”
Section: Resultsmentioning
confidence: 99%
“…the aberration (contributing one r / R lc ) and the retardation (contributing another r / R lc ). The symbol φ f denotes the absolute fiducial phase, determined by the detection of a photon emitted from the centre of the NS exactly at the moment when the dipole axis was in the ‐observer plane (see Dyks 2008 for details).…”
Section: The Phase‐dependent Effects Of Rotation On Pulsar Profilesmentioning
confidence: 99%
“…It is the inflection point of the IOF trajectory that is located at ( r cst , s cst ) [or ( r cst , θ cst )]. Thus, the region of the caustic pile‐up () is simultaneously the region of the zero‐curvature of electron trajectory in IOF, as localized by in Dyks (2008). By noting that one can rewrite in the form For a laterally extended emitter the zero (or minimum) curvature corresponds to the steepest gradient of the polarization angle swing.…”
Section: The Generation Of Asymmetric Profilesmentioning
confidence: 99%
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